We compared this PSF estimate with the values derived by convolution of the HST images for the F606W, F775W, F814W, and F850LP broadband filters. The method is identical to that used in the paper I [1]} for the MOSAIC and UDF-10 datacubes. For ease of comparison, a direct Moffat fit was performed on the M star for the four reconstructed HST broadband MUSE images. An additional comparison was performed by fitting a Moffat distribution to the average of all individual muse-psfr PSFs. The Moffat FWHM and \(\beta \)  shape parameter for the three different estimates are shown in the Table REF . Since the FWHM and \(\beta \)  parameters are not independent, we also provide the FWHM obtained by fitting a Gaussian profile to judge the difference in FWHM. However, we recall that the MUSE PSF is not well represented by a Gaussian function [2]}, [3]}.
As shown in Table REF , all methods give similar results with the expected decrease in FWHM with increasing wavelengths. However, there is a systematic offset between the methods: the HST convolution method overestimates the FWHM by \(\approx \) +0.05 arcsec while the muse-psfr method underestimates it by \(\approx \) -0.06 arcsec.
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